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Do maser stars trace a rotating Galactic bar?
Published online by Cambridge University Press: 01 March 2007
Abstract
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I have analyzed the radial velocities in two large samples of maser stars that cover the Galactic plane from l = +40deg to l = −40deg through the Galactic Centre. I compare a diagram of longitude versus radial velocity as observed with a diagram obtained from the calculation of orbits in a simple, but realistic potential containing a weak, rotating bar. Almost all stars belong to the Galactic disk but there is a small sample with high velocities close to the Galactic Centre and in the so-called forbidden quadrants. These velocities cannot be explained by a combination of pure Galactic rotation and a modest dispersion in velocity. An acceptable explanation is one in which the stars of this small sample move up and down a rotating Galactic bar.
- Type
- Contributed Papers
- Information
- Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 356 - 360
- Copyright
- Copyright © International Astronomical Union 2008
References
Garcia-Hernandez, D. A., Garcia-Lario, P., Plez, B., Manchado, A., D'Antona, F., Lub, J., & Habing, H. J. 2007, A&A 462, 711Google Scholar
Habing, H., Sevenster, M., Messineo, M., van der Ven, G., & Kuijken, K. 2006, A&A, 458, 151Google Scholar
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